Romer, A K, Becker, M R, Troxel, M A, MacCrann, N, Krause, E, Eifler, T F, Friedrich, O, Nicola, A, Refregier, A and The Dark Energy Collaboration, (2016) Cosmic shear measurements with Dark Energy Survey science verification data. Physical Review D, 94. 042005. ISSN 1550-7998

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Abstract

We present measurements of weak gravitational lensing cosmic shear two-point statistics using Dark Energy Survey Science Verification data. We demonstrate that our results are robust to the choice of shear measurement pipeline, either ngmix or im3shape, and robust to the choice of two-point statistic, including both real and Fourier-space statistics. Our results pass a suite of null tests including tests for B-mode contamination and direct tests for any dependence of the two-point functions on a set of 16 observing conditions and galaxy properties, such as seeing, airmass, galaxy color, galaxy magnitude, etc. We furthermore use a large suite of simulations to compute the covariance matrix of the cosmic shear measurements and assign statistical significance to our null tests. We find that our covariance matrix is consistent with the halo model prediction, indicating that it has the appropriate level of halo sample variance. We compare the same jackknife procedure applied to the data and the simulations in order to search for additional sources of noise not captured by the simulations. We find no statistically significant extra sources of noise in the data. The overall detection significance with tomography for our highest source density catalog is 9.7 sigma . Cosmological constraints from the measurements in this work are presented in a companion paper [DES et al., Phys. Rev. D 94, 022001 (2016).].

Item Type:	Article
Schools and Departments:	School of Mathematical and Physical Sciences > Physics and Astronomy
Research Centres and Groups:	Astronomy Centre
Subjects:	Q Science > QB Astronomy
Depositing User:	Richard Chambers
Date Deposited:	28 Nov 2016 08:18
Last Modified:	02 Jul 2019 18:37
URI:	http://sro.sussex.ac.uk/id/eprint/65679

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